TOI-1416: A system with a super-Earth planet with a 1.07 d period
TOI-1416: A system with a super-Earth planet with a 1.07 d period
复制标题
TOI-1416：一个拥有周期为 1.07 d 的超级地球行星的系统
DOI：
10.1051/0004-6361/202346370
复制
发表时间：
2023
影响因子：
6.5
通讯作者：
Deeg H
中科院分区：
文献类型：
--
作者：
Deeg H
TOI-1416（BD+42 2504，HIP 70705）是一颗V =10的晚G型或早K型矮星星星。TESS在其第16、23和50扇区探测到过境，深度约为455 ppm，周期为1.07天。径向速度（RV）证实了凌日行星TOI-1416 b的存在，它的质量为3.48 ± 0.47 M <$，半径为1.62 ± 0.08 R <$，这意味着它的密度略低于地球，为4.50−0.83+ 0.99 g cm−3。RV数据还进一步显示了一颗周期为27.4或29.5天的行星c，其性质无法证实，因为强烈怀疑受到与月球29.53天会合周期相关的信号的污染。近超短周期行星TOI-1416是短周期高温类地行星的典型代表。一个含有大量溶解水的熔融岩浆内部的行星模型为其成分提供了一个合理的解释，其大气层可能适合JWST的透射光谱。TOI-1416 b在半径周期分布中的位置证实了周期小于一天的行星不会形成任何特殊的群。这意味着超短周期行星属于一个连续分布的超类地行星，其周期从已知最短的到2030天不等;它们的周期半径分布被海王星沙漠和周期半径谷所界定，后者将超级地球与次海王星行星分开。在大量的小型短周期行星中，在0.6-1.4天的周期之间出现了一个显著的平台，这与低离心率形成通道相一致。对于海王星沙漠，由于短周期行星数量的增加，它的下限需要修改;对于短于2天的周期，我们确定半径为1.6 R <$p，质量为0.028 Mjup（相当于8.9 M <$p）作为沙漠的下限。我们还提供了相应的限制海王星沙漠对行星的日照和有效温度。
TOI-1416 (BD+42 2504, HIP 70705) is aV=10 late G- or early K-type dwarf star. TESS detected transits in its Sectors 16, 23, and 50 with a depth of about 455 ppm and a period of 1.07 days. Radial velocities (RVs) confirm the presence of the transiting planet TOI-1416b, which has a mass of 3.48 ± 0.47M⊕and a radius of 1.62 ± 0.08R⊕, implying a slightly sub-Earth density of 4.50−0.83+0.99g cm−3. The RV data also further indicate a tentative planet,c, with a period of 27.4 or 29.5 days, whose nature cannot be verified due to strong suspicions of contamination by a signal related to the Moon’s synodic period of 29.53 days. The nearly ultra-short-period planet TOI-1416bis a typical representative of a short-period and hot (Teq≈ 1570 K) super-Earth-like planet. A planet model of an interior of molten magma containing a significant fraction of dissolved water provides a plausible explanation for its composition, and its atmosphere could be suitable for transmission spectroscopy with JWST. The position of TOI-1416bwithin the radius-period distribution corroborates the idea that planets with periods of less than one day do not form any special group. It instead implies that ultra-short-period planets belong to a continuous distribution of super-Earth-like planets with periods ranging from the shortest known ones up to ≈30 days; their period-radius distribution is delimited against larger radii by the Neptune Desert and by the period-radius valley that separates super-Earths from sub-Neptune planets. In the abundance of small, short-periodic planets, a notable plateau has emerged between periods of 0.6–1.4 days, which is compatible with the low-eccentricity formation channel. For the Neptune Desert, its lower limits required a revision due to the increasing population of short-period planets; for periods shorter then 2 days, we establish a radius of 1.6R⊕and a mass of 0.028Mjup(corresponding to 8.9M⊕) as the desert’s lower limits. We also provide corresponding limits to the Neptune Desert against the planets’ insolation and effective temperatures.